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Modeling Extreme Mass Ratio Inspirals within the Effective-One-Body Approach

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arxiv 0909.4263 v2 pith:GWJMJCOV submitted 2009-09-23 gr-qc astro-ph.COastro-ph.GAastro-ph.HE

Modeling Extreme Mass Ratio Inspirals within the Effective-One-Body Approach

Nicolas Yunes , Alessandra Buonanno , Scott A. Hughes , M. Coleman Miller , Yi Pan This is my paper
classification gr-qc astro-ph.COastro-ph.GAastro-ph.HE
keywords inspiralsapproachdifferenceeffective-one-bodyevolutioninclusionlessmodeling
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We present the first models of extreme-mass-ratio inspirals within the effective-one-body (EOB) formalism, focusing on quasi-circular orbits into non-rotating black holes. We show that the phase difference and (Newtonian normalized) amplitude difference between analytical EOB and numerical Teukolsky-based gravitational waveforms can be reduced to less than 10^(-1) rad and less than 2 x 10^(-3), respectively, after a 2-year evolution. The inclusion of post-Newtonian self-force terms in the EOB approach leads to a phase disagreement of roughly 6-27 rad after a 2-year evolution. Such inclusion could also allow for the EOB modeling of waveforms from intermediate-mass ratio, quasi-circular inspirals.

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    A closed-form Kerr metric under slow quadrupolar tides yields spin-dependent tidal shifts of the ISCO and light ring, with larger shifts for retrograde orbits around fast-spinning holes.